Identification of an X-Ray Pulsar in the BeXRB System IGR J18219-1347

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dc.citation.articleNumber139en_US
dc.citation.issueNumber2en_US
dc.citation.journalTitleThe Astrophysical Journalen_US
dc.citation.volumeNumber927en_US
dc.contributor.authorO'Connor, B.en_US
dc.contributor.authorGöğüş, E.en_US
dc.contributor.authorHuppenkothen, D.en_US
dc.contributor.authorKouveliotou, C.en_US
dc.contributor.authorGorgone, N.en_US
dc.contributor.authorTownsend, L.J.en_US
dc.contributor.authorCalamida, A.en_US
dc.contributor.authorFruchter, A.en_US
dc.contributor.authorBuckley, D.A.H.en_US
dc.contributor.authorBaring, M.G.en_US
dc.contributor.authorKennea, J.A.en_US
dc.contributor.authorYounes, G.en_US
dc.contributor.authorArzoumanian, Z.en_US
dc.contributor.authorBellm, E.en_US
dc.contributor.authorCenko, S.B.en_US
dc.contributor.authorGendreau, K.en_US
dc.contributor.authorGranot, J.en_US
dc.contributor.authorHailey, C.en_US
dc.contributor.authorHarrison, F.en_US
dc.contributor.authorHartmann, D.en_US
dc.contributor.authorKaper, L.en_US
dc.contributor.authorKutyrev, A.en_US
dc.contributor.authorSlane, P.O.en_US
dc.contributor.authorStern, D.en_US
dc.contributor.authorTroja, E.en_US
dc.contributor.authorHorst, A.J. van deren_US
dc.contributor.authorWijers, R.A.M.J.en_US
dc.contributor.authorWoudt, P.en_US
dc.date.accessioned2022-04-15T14:45:22Zen_US
dc.date.available2022-04-15T14:45:22Zen_US
dc.date.issued2022en_US
dc.description.abstractWe report on observations of the candidate Be/X-ray binary (BeXRB) IGR J18219−1347 with the Swift/X-ray Telescope, the Nuclear Spectroscopic Telescope ARray, and the Neutron Star Interior Composition Explorer during Type-I outbursts in 2020 March and June. Our timing analysis revealed the spin period of a neutron star with P spin = 52.46 s. This periodicity, combined with the known orbital period of 72.4 days, indicates that the system is a BeXRB. Furthermore, by comparing the spectral energy distribution of the infrared counterpart to that of known BeXRBs, we confirm this classification and set a distance of approximately 10–15 kpc for the source. The broadband X-ray spectrum (1.5–50 keV) of the source is described by an absorbed power law with a photon index Γ ∼ 0.5 and a cutoff energy at ∼13 keV.en_US
dc.identifier.citationO'Connor, B., Göğüş, E., Huppenkothen, D., et al.. "Identification of an X-Ray Pulsar in the BeXRB System IGR J18219-1347." <i>The Astrophysical Journal,</i> 927, no. 2 (2022) IOP Publishing: https://doi.org/10.3847/1538-4357/ac5032.en_US
dc.identifier.digitalOConnor_2022_ApJ_927_139en_US
dc.identifier.doihttps://doi.org/10.3847/1538-4357/ac5032en_US
dc.identifier.urihttps://hdl.handle.net/1911/112076en_US
dc.language.isoengen_US
dc.publisherIOP Publishingen_US
dc.rightsOriginal content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.en_US
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/en_US
dc.titleIdentification of an X-Ray Pulsar in the BeXRB System IGR J18219-1347en_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
dc.type.publicationpublisher versionen_US
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